Аннотация
We report results from a convection dynamo simulation of proto-neutron star
(PNS), with a nuclear equation of state (EOS) and the initial hydrodynamic
profile taken from a neutrino radiation-hydrodynamics simulation of a massive
stellar core-collapse. A moderately-rotating PNS with the spin period of $170$
ms in the lepton-driven convection stage is focused. We find that large-scale
flow and thermodynamic fields with north-south asymmetry develop in the
turbulent flow, as a consequence of the convection in the central part of the
PNS, which we call as a "deep core convection". Intriguingly, even with such a
moderate rotation, large-scale, $10^15$ G, magnetic field with dipole
symmetry is spontaneously built up in the PNS. The turbulent electro-motive
force arising from rotationally-constrained core convection is shown to play a
key role in the large-scale dynamo. The large-scale structures organized in the
PNS may impact the explosion dynamics of supernovae and subsequent evolution to
the neutron stars.
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